【摘要】 用一个简洁的方法推出辐射亮度相对论性变换关系 对于热辐射 ,在光学厚和光学薄的情况下 ,一个温度为T ,视向运动速度为 βμ的天体 ,其观测温度都是为 [γ(1- βμ) ]- 1T ,即向着观测者运动的天体所观测的热辐射温度要比它远离观测者时高 ;而对于高同步加速非热辐射 ,在光学薄的情况下 ,辐射强度变化因子为γ[γ(1 βμ) ]- 3-α,而在光学厚的情况下 ,变因子为γ(1- βμ) - 1/2 类似地 ,向着观测者运动的天体所观测的非热辐射强度要高于其他运动方向的天体的辐射强度更多还原

【Abstract】 Modern astrophysical observations with large telescopes and sensitive detects have allowed us to explore the very deep universe. Galaxies and quasars with the redshift Z=4 and greater are found. Observed intensities and spectrum must be misrepresented, enhanced or suppressed by the relativistic Doppler effect. So, relativistic effect on the radiative transfer must be considered for emission from these high red-shift objects such. A simple and direct derivation for the relativistic transformation of the brightness is presented in the paper. For the free-free emission with both optical thin and opaque, the observed brightness temperature is boosted or attenuated by the factor [ γ(1-βμ′ )] -1 . For the optical thin and opaque synchrotron emission, the factors are γ[γ(1-βμ′ )] -3-α and [ γ(1-βμ′ )] -1/2 , respectively. The intensities of the approaching objects are enhanced by the factors and of the receding one are suppressed by the factors.更多还原